Infrared Emission from Interstellar Dust. III. The Small Magellanic Cloud

The infrared (IR) emission from interstellar dust in the Small Magellanic Cloud (SMC) is modelled using a mixture of amorphous silicate and carbonaceous grains, including a population of PAH molecules. (1) The IR spectrum of the quiescent molecular cloud SMC B1#1 can be reproduced by our dust model provided the PAH mixture has intrinsic IR band strengths which differ from the band strengths which best fit Milky Way PAH mixtures. The variation in the PAH IR band strengths may be a consequence of the differing metallicity or environmental conditions. (2) The dust model is also able to reproduce the spectral energy distribution from near-IR to far-IR for the SMC B1#1 cloud, as well as for the entire SMC Bar region. The general SMC Bar region must have a much lower PAH abundance than in the SMC B1#1 cloud.

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